Florencia Jiménez Luján Status of the field Optical range BAL QSO meeting 2009 Jun 24 – 26 Bologna (Italy)

STATUS OF THE FIELD - OPTICAL RANGE BAL QSO meeting 2009 – Jun , Bologna (Italy)Florencia Jiménez Luján 2 arXiv:astro-ph/ Evolutionary and composite model for AGNs. Orientation/obscuration effects take the role of a second parameter providing the segregation between Sy1/Sy2 and BLRG/NLRG. SMBH (Super massive black hole) + SB (starburst) with OF (outflows) 1.Young AGN are obscured BAL and strong Fe II emitters with relatively narrow line BLR and a compact and faint NLR; their radio emission is also compact. 2.Old AGN are weak Fe II emitters with broad line BLR and extended and bright NLR and fully developed radio lobes. 3.The orientation of the AGN/toroid takes the role of a second parameter providing the segregation between type1/type2, and BLRG/NLRG.

STATUS OF THE FIELD - OPTICAL RANGE BAL QSO meeting 2009 – Jun , Bologna (Italy)Florencia Jiménez Luján 3 arXiv:astro-ph/ i.BALs are young systems with composite outflows. ii.The Fe II intensity provides an age indicator for BLR AGNs. iii.BLR emission line FWHM change with age. iv.X-ray slope changes with age. v.[O III] intensity and FWHM changes with age. vi.The strong IR continuum emission is associated with the composite nuclear nature. vii.The Sy1/Sy2 and BLRG/NLRG segregation is mainly due to orientation/obscuration by toroid.

STATUS OF THE FIELD - OPTICAL RANGE BAL QSO meeting 2009 – Jun , Bologna (Italy)Florencia Jiménez Luján 4 arXiv:astro-ph/ BALs (SDSS DR3) BALs may have broader emission lines on average than other quasars (disk-like configuration). Cosmology: Ω M = 0.3, Ω Λ = 0.7, H 0 = 70 km s -1 Mpc -1

STATUS OF THE FIELD - OPTICAL RANGE BAL QSO meeting 2009 – Jun , Bologna (Italy)Florencia Jiménez Luján 5 arXiv:astro-ph/ BALs (SDSS); 3 strongly variable BALs (the strongest BAL variability occurs among the smallest equivalent width features and at velocities exceeding km s -1 ). CIV < 1 year BALs primarily vary in depth on those timescales. Some changes in velocity width. The dominant contribution to the BAL variability is a changing degree of ionisation or covering factor. The infrequency of observed changes in velocity likely reflects the very long timescales on which these features can be seen to accelerate.

STATUS OF THE FIELD - OPTICAL RANGE BAL QSO meeting 2009 – Jun , Bologna (Italy)Florencia Jiménez Luján 6 arXiv: Spitzer MIPS (24, 70 and 160 µm) The mid-infrared properties of BALs are consistent with those of non-BALs of comparable luminosity. BALs typically show more evidence for dust reddening and extinction in their ultraviolet-optical spectra. BALs are remarkably weak X-ray emitters Cosmology: Ω M = 0.3, Ω Λ = 0.7, H 0 = 70 km s -1 Mpc -1

STATUS OF THE FIELD - OPTICAL RANGE BAL QSO meeting 2009 – Jun , Bologna (Italy)Florencia Jiménez Luján 7 arXiv: quasars (SDSS DR2) While quasars accreting near the Eddington limit are more likely to show BALs than lower L/L Edd systems, BALs are present in quasars accreting at only a few percent Eddington. The most (bolometric) luminous quasars are more likely to show BALs. BALs are redder on average than unabsorbed quasars. The outflow acceleration has to be due to ultraviolet line scattering (upper envelope). However, many BALs terminate at small velocities which may indicate the importance of wind-orientation, or non-radiative processes in driving outflows. Cosmology: Ω M = 0.3, Ω Λ = 0.7, H 0 = 70 km s -1 Mpc -1

STATUS OF THE FIELD - OPTICAL RANGE BAL QSO meeting 2009 – Jun , Bologna (Italy)Florencia Jiménez Luján 8 arXiv: AGN outflows are common and important: i.chemical enhancement of the interstellar and intergalactic media ii.angular momentum removal from the accreting central engine iii.limiting star formation in starburst systems by blowing out gas and dust from the host galaxy Cosmology: Ω M = 0.3, Ω Λ = 0.7, H 0 = 70 km s -1 Mpc -1 FRACTION ~ 60 %

STATUS OF THE FIELD - OPTICAL RANGE BAL QSO meeting 2009 – Jun , Bologna (Italy)Florencia Jiménez Luján 9 arXiv: BALs (3 - 6 years): Variation produced by changes in outflow geometry No significant changes in the BAL onset velocity: absorber is far from the source absorber is being continually replenished and is azimutally symmetric few thousand km s -1 ; absoption depth is ≤ 25 % |ΔEW/ | ~ 0.3 Cosmology: Ω M = 0.3, Ω Λ = 0.7, H 0 = 72 km s -1 Mpc -1 BALs could have lifetimes as short as a few decades changes: outflow structures variation of covering factor no acceleration

STATUS OF THE FIELD - OPTICAL RANGE BAL QSO meeting 2009 – Jun , Bologna (Italy)Florencia Jiménez Luján 10 arXiv: ~ 4200 BAL (SDSS DR5) No significant difference between the clustering strengths of BALs and non-BALs. Their clustering results suggest that BALs live in similar large-scale environments as do non-BALs. It may still be that members of the rare subclass FeLoBALs are intrinsically differentfrom ordinary quasars and may reside in different environments (not sampled enough). Cosmology: Ω M = 0.26, Ω Λ = 0.74, H 0 = 71 km s -1 Mpc -1

STATUS OF THE FIELD - OPTICAL RANGE BAL QSO meeting 2009 – Jun , Bologna (Italy)Florencia Jiménez Luján 11 arXiv: SDSS (DR3) Observed: ~ 13.5 % upper limit: 18.3 % Intrinsic: ~ 17 % f (BALs) = 0.17 ± 0.01 (stat) ± 0.03 (sys) upper limit: f(BALs) ~ 0.23

STATUS OF THE FIELD - OPTICAL RANGE BAL QSO meeting 2009 – Jun , Bologna (Italy)Florencia Jiménez Luján 12 arXiv: quasars (SDSS DR5) Strong correlation between the EW(CIV) and the continuum luminosity. Up to z ~ 5, the slope of the Baldwin Effect seems to have no effect of cosmological evolution. EW(CIV) have a strong correlation with the mass of supermassive black hole (SMBH) and a weak correlation with the Eddington ratio L Bol /L Edd. This suggest that the SMBH mass is probably the primary drive for the Baldwin Effect.

STATUS OF THE FIELD - OPTICAL RANGE BAL QSO meeting 2009 – Jun , Bologna (Italy)Florencia Jiménez Luján 13 J z ~ 2.1 CIV + SiIV FWHM ~ 4000 km s -1 v ~ km s % covering size ~ 4 x cm column density N H (cm -2 ) ≥ 21.2 average space density n H ≥ 2 x 10 5 cm -2 It due to changes in the ionisation (unlikely) or due to movement of gas across our lines of sight. arXiv:

STATUS OF THE FIELD - OPTICAL RANGE BAL QSO meeting 2009 – Jun , Bologna (Italy)Florencia Jiménez Luján BALs optically selected velocity range (trough) ≥ 2000 km/s velocities – 0 km/s SiIV, CIV, AlIII, Mg II (different shapes ion-dependent structure in the outflow) Chandra + XMM-Newton Cosmology: Ω M = 0.3, Ω Λ = 0.7, H 0 = 70 km s -1 Mpc -1 arXiv:

STATUS OF THE FIELD - OPTICAL RANGE BAL QSO meeting 2009 – Jun , Bologna (Italy)Florencia Jiménez Luján 15 1.BALs are more strongly reddened in the rest-frame UV than non-BALs (LoBALs are even redder than HiBALs). 2.BALs are relatively X-ray weak compared to non-BALs. 3.The observed BAL fraction is dependent on the spectral S/N (high S/N ~ 15 %). 4.BALs show a similar Baldwin effect as for non-BALs (EW(CIV) decreases with increasing continuum luminosity). BALs have weaker CIV emission in general than do non-BALs. 5.BALs are weaker at a wide range of velocities and stronger at lower outflow velocities. 6.BAL outflow velocity and UV absorption strength are correlated with relative X-ray weakness. Sources with higher UV luminosities are more likely to have higher-velocities outflows (radiation pressure accelerates BAL outflows, but in low S/N sources those high velocities can be obscured). 1-6: in qualitative agreement with models that depend on strong X-ray absoption to shield the outflow from over-ionisation and enable radiative acceleration. arXiv:

STATUS OF THE FIELD - OPTICAL RANGE Appendix BAL QSO meeting 2009 – Jun , Bologna (Italy)Florencia Jiménez Luján 16 Different definitions: BALnicity index (Weymann et al. 1991):Weymann et al minimum width = 2000 km s -1 only CIV BI Absorption index (Hall et al. 2002):Hall et al minimum width = 450 km s -1 any multiplet AI Gibson et al arXiv: Lower limit: 3000 km s -1 0 km s -1 any multiplet Trump et al arXiv:astro-ph/ Upper limit: km s km s -1 CIV and MgII